10-Minute cadence proton and helium spin-averaged coincidence fluxes from the
COSPIN Anisotropy Telescopes (AT1 and AT2). The two telescopes differ only by their orientation
with respect to the spacecraft spin axis. The parameter keys in the parameter-level segments below are specifically relevant to the UFA-accessible versions of the data.

A directory containing daily ftp-downloadable files containing readout-by-readout
listings of HET housekeeping paramaters (Voltages, Temperatures, Offsets).
The naming convention of the files is uly_het_full_house_YYYDDD.txt, where YYY
indicates the three-digit year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for
2002) and DDD indicates the three digit day of year (Jan. 1 = 1).
In each file, following a detailed description of the format, the data consist of a
a listing of HET housekeeping parameters measured at the time listed in the first
4 columns of each line. Each line contains data for one readout of the parameters.
The first 4 columns give the time of the measurement as fractional year (to 12
decimal places) and as year since 1900, day of year, and ms of day.
At the most common science telemetry rate, 2048 bps, each parameter in this file
is read out once every 256 seconds. The measurements are instantaneous, and do
not represent an average of values over the interval since the last readout.
The sole function of these parameters is to monitor instrument health.
No noise-removal or despiking has been done, so caution must be used in
interpreting isolated large increases or decreases in the measured parameters.

A directory containing daily ftp-downloadable files containing full information for
every non-zero HET pulse-height event returned in telemetry, including raw channels
and discriminator states, the energy deposits corresponding to the channels, and certain
derived quantities including particle charge and trajectory through the telescope.
Pulse height analysis is performed for electrons and nuclei with penetrating power
equivalent to that of protons with energy greater than 14 MeV.
The naming convention of the files is uly_het_full_pha_YYYDDD.txt, where YYY indicates
the three-digit year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for 2002) and DDD
indicates the three digit day of year (Jan. 1 = 1).
At the start of each file there isa detailed description of the format, in which each
event is represented by a line with 54 columns that provide complete information
about the event.
The first 4 columns give the time of the opening of the window in which the event
was recorded as fractional year (to 12 decimal places) and as year since 1900,
day of year, and ms of day. At the most common science telemetry rate, 2048 bps,
six events are collected in every 32 second telemetry format. Because of the large
geometrical factor of the telescope, almost every available pha slot contains an
event. Since far more events are recorded in the telescope than can be returned
as pha events in the telemetry, only a sample of the events incident on the telescope
can be sent down as pha events.
With the pha data for an event, the particle's charge, mass, kinetic energy, and
trajectory through the telescope can be determined. While most of the nuclei incident
on the HET are protons, a three-level priority system selects events for pulse-height
analyis and return in the telemetry so as to assure capture of almost all of the
relatively rare heavy element nuclei that stop in the telescope. The lowest priority
(P3) events are those that satisfy the most basic criteria for being an analyzable event,
as determined by the combination of discriminators on various detectors in the telescope
that fire. A higher priority (P2) is given to events that stop in the telescope, and the
highest priority (P1) is given to events that stop in the telescope and that are identified
as heavy nuclei by the size of their energy deposits in the detectors.
The highest priority event that occurs in each window for accumulation of pha events
is selected for inclusion in the telemetry data returned to the ground. Thus, in large
solar energetic particle events with abundant heavy nuclei, few protons may be included
in the pha events transmitted via telemetry. The counting rates, however, count every
event, and in such cases it can usually be assumed the counting rates that respond to
protons are dominated by the proton flux.
Absolute fluxes for individual elements may be derived by identifying pha events that
would contribute to counting rates (i.e. that have the same discriminator configuration as
one of the counting rates) and determining the ratio between events counted by the rate
and returned in telemetry during a given interval. Appropriate counting rates exist
that match each of the three pha priority states. The priority levels corresponding to the
counting rates are listed in Table 7 of Simpson et al. (Astron. Astrophys., 92, 365-399, 1972).
*** N.B. Three corrections are necessary in Table 7 of Simpson et al. (1972). ***
1) The (H) discrimator logic should include the discriminator K6H orred with the other
seven discriminators listed.
2) the middle term of the P2 (medium priority) logic should include D4 as well as
D1, D2, and D6 as required detectors.
3) Because of an error in the logic design counting rate H3, listed as responding to
P3 (lowest priority) events, also includes P2 events which satisfy the first term
in the P2 logic. Thus H3 should not be used for deriving absolute fluxes of P3
events from PHA data.

A directory containing daily ftp-downloadable files containing readout-by-readout listings of
the counts accumulated in the H1-H9 spin-averaged counting rates. These counting rates respond
primarily to protons (H1-H5, H9) in the approximate energy ranges 5.4-14, 14-19, 24-31, 34-68,
68-92, and >92 MeV, respectively, and to electrons (H6-8) in the very approximate energy ranges
1-3, 5-10, and 3-5 MeV, respectively.
The naming convention for the daily files is uly_het_full_rat_omni1_YYYDDD.txt, where YYY
indicates the three-digit year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for 2002) and
DDD indicates the three digit day of year (Jan. 1 = 1).
In each file, following a detailed description of the format, the data consist of a
listing of counts accumulated in the H1-H9 spin-averaged counting rates during the intervals
between successive readouts, organized into columns as described below.
The first 4 columns give the start time of the counting rate accumulation period as
fractional year (to 12 decimal places) and as year since 1900, day of year, and ms
of day at the start of the accumulation, followed by 1 column giving the duration of
the accumulation period in milli-seconds (it is the same for all 9 rates), and 9
columns giving the counts accumulated in that period for each rate. All fields
except for the fractional year are in integer format.
Each line contains data for one single readout of the rates H1-H9, and all readouts
where at least one of the rates has a non-fill value are included. Where fill
does occur it is indicated by -1.
Since the accumulation period for each readout is forced to include an integral number
of spacecraft spins in order to produce pure spin-averaged measurements, the lengths of
the accumulation periods vary in a cyclic manner as the period of the telemetry cycle
beats with the spacecraft spin period. All counting rates in this file are read out
twice per spacecraft format. At the most common science telemetry bit rate (2048 bps)
this corresponds to an average interval between readouts of 16 seconds. Thus, with a
typical 5 rpm spacecraft spin rate the accumulation intervals vary in a repeating cycle of
12, 12, 24, 12, 12, 24, 12, etc. seconds. At lower bit rates the average interval is
equal to 16x(2048/BR) seconds and the cycle automatically adjusts to produce this average
accumulation.
No noise-removal or despiking has been done, so caution must be used in interpreting isolated
large increases or decreases in the counting rates.

A directory containing daily ftp-downloadable files containing readout-by-readout listings of
the counts accumulated in the H1-H27 spin-averaged counting rates. The rates H10-H13 are
coincidence counting rates corresponding primarily to heavy nuclei (Z>2) with penetrating
power equivalent to carbon-12 nuclei in the approximate energy ranges 26-36, 44-127, 127-173,
and >173 MeV/nucleon, resspectively.
H14-H27 are single detector counting rates giving, in order, the total number of counts
above the lowest level discriminator thresholds of detectors D1-D6, K1-K6 (or D7-D12),
A (or D13), and the anti-coincidence scintillator S. The single detector counting rates
are provided simply to assess the health of the detectors and are of little use
scientifically.
The naming convention for the daily files is uly_het_full_rat_omni2_YYYDDD.txt, where YYY
indicates the three-digit year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for 2002) and
DDD indicates the three digit day of year (Jan. 1 = 1).
In each file, following a detailed description of the format, the data consist of a listing
of counts accumulated in the H10-H27 spin-averaged counting rates during the intervals
between successive readouts, organized into columns as described below.
The first 4 columns give the start time of the counting rate accumulation period as
fractional year (to 12 decimal places) and as year since 1900, day of year, and ms
of day at the start of the accumulation, followed by 1 column giving the duration of
the accumulation period in milli-seconds (it is the same for all rates except H13,
which is read out twice in each accumulation period, and is thus represented as
H13a and H13b - see below and embedded documentation in each daily file), and 19
columns giving the counts accumulated in that period for each rate. All fields
except for the fractional year are in integer format. The start time for H13a is
the time given as the start time for the line, but (to sufficient accuracy) its
accumulation period is half the period given under "coverage". Again, to sufficient
accuracy, the start time for H13b is the time given plus half the accumulation period,
and the accumulation period for H13b is half the period given under "coverage".
Each line contains data for one single readout of the rates H10-H12, H13a,
H13b, and H14-H27. All readouts where at least one of the rates has a non-fill value
are included. Where fill does occur it is indicated by -1.
Since the accumulation period for each readout is forced to include an integral number
of spacecraft spins in order to produce pure spin-averaged measurements, the lengths of
the accumulation periods vary in a cyclic manner as the period of the telemetry cycle
beats with the spacecraft spin period. At the most common science telemetry rate,
2048 bps, each rate in this file is read out on average once every 128 seconds, except for
H13 which is readout on average twice in every 128 seconds. At 2048 bps, the cycle of
accumulation periods is 132, 132, 120, 132, 132,, 120, 132, ... seconds.
No noise-removal or despiking has been done, so caution must be used in
interpreting isolated large increases or decreases in the counting rates.

A directory containing daily ftp-downloadable files containing readout-by-readout listings
of the counts accumulated in each spin-sector of the 8-sectored H7S counting rate. Aside
from its division of counts into spin-sectors, H7S is a coincidence counting rate with
coincidence logic requirements identical to the spin-averaged counting rate H7. Therefore
both the H7 and the H7S counting rates respond primarily to electrons in the very approximate
energy range ~5-10 MeV.
The naming convention for the daily files is uly_het_full_rat_sect1_YYYDDD.txt, where YYY
indicates the three-digit year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for 2002) and
DDD indicates the three digit day of year (Jan. 1 = 1).
In each file, following a detailed description of the format, the data consist of a
readout by readout listing of counts accumulated in the eight 45 degree spin sectors
of the sectored counting rate H7S during the intervals between successive readouts, organized
into columns as described below.
The first 4 columns give the start time of the counting rate accumulation period for
sector 7 of the rate as fractional year (to 12 decimal places) and as year since 1900,
day of year, and ms of day at the start of the accumulation, followed by 1 column (labeled
cov) giving the duration of the total accumulation period for all 8 sectors in
milli-seconds. Thus the accumulation period in each of the sectors is the value given
in the "cov" column divided by 8. The accumulation in each of the successive sectors
7,8,1,2,3,4,5, and 6 starts cov/8 milliseconds after the start of the accumulation in
the previous sector. Columns 6-13 then give the counts accumulated in each of the
eight sectors during the accumulation period.
Each line contains data for one single readout accumulation of the 8 sectors of H7S.
Since the accumulation period for each readout is forced to include an integral number
of spacecraft spins in order to produce equal coverage in all sectors, the lengths of
the accumulation periods vary in a cyclic manner as the period of the telemetry cycle
beats with the spacecraft spin period.
The H7S counting rate is fully read out every 64 seconds at the most common science
telemetry bit rate (2048 bps). Thus, with a typical 5 rpm spacecraft spin rate the
accumulation intervals vary in a repeating cycle of 60, 60, 72, 60, 60, 72, 60, etc.
seconds. At lower bit rates the average interval is equal to 64x(2048/BR) seconds
and the cycle automatically adjusts to produce this average accumulation.
The spin plane of the Ulysses spacecraft, in which the sectors are defined, is
normal to the spin axis (spacecraft +Z axis), which is maintained within 1-2 degrees
of Earth-pointing at all times. Viewed from Earth the spacecraft spins counter-clockwise.
The start of sector 1 is defined by the spacecraft-generated Sun Pulse, which is issued
when the sun crosses the +X/+Z quadrant of the X/Z plane. The HET telescope axis is
parallel to the +X axis and normal to the Z axis.
No noise-removal or despiking has been done, so caution must be used in
interpreting isolated large increases or decreases in the counting rates.

A directory containing daily ftp-downloadable files containing readout-by-readout listings
of the counts accumulated in each spin-sector of the 8-sectored H45S counting rate. Aside
from its division of counts into spin-sectors, H45S is a coincidence counting rate with
coincidence logic requirements satisfying the logical inclusive OR of the H4 and H5 spin-
averaged counting rates. Therefore the H45S counting rate responds primarily to protons
in the approximate energy range 34-92 MeV.
The naming convention for the daily files is uly_het_full_rat_sect2_YYYDDD.txt, where YYY
indicates the three-digit year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for 2002) and
DDD indicates the three digit day of year (Jan. 1 = 1).
In each file, following a detailed description of the format, the data consist of a
readout by readout listing of counts accumulated in the eight 45 degree spin sectors
of the sectored counting rate H45S during the intervals between successive readouts, organized
into columns as described below.
The first 4 columns give the start time of the counting rate accumulation period for
sector 7 of the rate as fractional year (to 12 decimal places) and as year since 1900,
day of year, and ms of day at the start of the accumulation, followed by 1 column (labeled
cov) giving the duration of the total accumulation period for all 8 sectors in
milli-seconds. Thus the accumulation period in each of the sectors is the value given
in the "cov" column divided by 8. The accumulation in each of the successive sectors
7,8,1,2,3,4,5, and 6 starts cov/8 milliseconds after the start of the accumulation in
the previous sector. Columns 6-13 then give the counts accumulated in each of the
eight sectors during the accumulation period.
Each line contains data for one single readout accumulation of the 8 sectors of H45S.
Since the accumulation period for each readout is forced to include an integral number
of spacecraft spins in order to produce equal coverage in all sectors, the lengths of
the accumulation periods vary in a cyclic manner as the period of the telemetry cycle
beats with the spacecraft spin period.
The H45S counting rate is fully read out every 128 seconds at the most common science
telemetry bit rate (2048 bps). Thus, with a typical 5 rpm spacecraft spin rate the
accumulation intervals vary in a repeating cycle of 132, 132, 120, 132, 132, 120, etc.
seconds. At lower bit rates the average interval is equal to 128x(2048/BR) seconds
and the cycle automatically adjusts to produce this average accumulation.
The spin plane of the Ulysses spacecraft, in which the sectors are defined, is
normal to the spin axis (spacecraft +Z axis), which is maintained within 1-2 degrees
of Earth-pointing at all times. Viewed from Earth the spacecraft spins counter-clockwise.
The start of sector 1 is defined by the spacecraft-generated Sun Pulse, which is issued
when the sun crosses the +X/+Z quadrant of the X/Z plane. The HET telescope axis is
parallel to the +X axis and normal to the Z axis.
No noise-removal or despiking has been done, so caution must be used in
interpreting isolated large increases or decreases in the counting rates.

Daily average PHA-based proton and helium fluxes and errors from the
COSPIN High Energy Telescope (HET) in the approximate energy ranges
39-70 MeV/n and 71-94 MeV/n from Day 296, 1990 through Day 181, 2009

10-Minute average ion and electron spin-averaged coincidence counting rates from the
COSPIN High Energy Telescope (HET). The parameter keys in the parameter-level segments below are specifically relevant to the UFA-accessible versions of the data.

10-Minute average ion and electron 8-sectored coincidence counting rates from the COSPIN High Energy Telescope (HET). These data provide a measure of the anisotropy of particle arrival directions in the spacecraft spin plane

Nominal 10 minute average spin-averages and sectored counting-rate-based fluxes of energetic protons and heavier
nuclei from the Ulysses COSPIN High Flux Telescope. The parameter keys in the parameter-level segments below are specifically relevant to the UFA-accessible versions of the data.

This data set contains information collected by the Ulysses Cosmic Dust instrument on the dust environment in interplanetary space within the inner solar system, between Jupiter and the Sun, and at high polar latitudes of the Sun. Both interplanetary and interstellar dust particles have been detected. This information is collected with a dust impact experiment, from which may be inferred direction of motion, mass, velocity and charge (see ULYDINST.CAT). The data presented in this dataset include instrumental readouts, inferred metadata, calibration information and a calendar of events.

This trajectory data set is provided by NSSDC. NSSDC has been actively supporting the Ulysses mission from the start by providing up-to-date trajectory-related data and graphics to the investigator community and the cognizant NASA Headquarters personnel. Soon after the launch, NSSDC generated (and later updated after Jupiter encounter) and loaded online for public access a list file of daily coordinates for Ulysses, along with software to manipulate these Cartesian coordinates into other sets, notably the heliographic latitude/longitude/radial distance. Similar online files of all other heliospheric spacecraft enable computations of their relative locations. The NSSDC Report 91-08, "Trajectories of Inner and Outer Heliospheric Spacecraft," has been requested often. (Higher resolution data may be obtained by executing the online code in DECnet: RUN NSSDCA::ANON_DIR:[ACTIVE.HELIO]HELICOOR.

This data set contains high resolution samples at about one-minute intervals of the interplanetary magnetic field measured by the Ulysses Magnetic Field experiment. Field vector components are given in units ofnanoteslas and in RTN coordinates, where R is the radial component or the sun-s/c axis, T is the transverse (along-track) component or the cross product of the solar rotation axis and R, and N is the normal (cross-track) component or the cross product of R and T. The field magnitudes in nT are averages of scalar magnitudes at higher time resolution. Times are computed at the mid-point of each
minute interval and expressed in Spacecraft Event Time - UT (SCET-UT). Data gaps have not been flagged in any way - if there were no available data in a particular hour then there is no data record for that hour. No data from the Feb. 1992 encounter with Jupiter are included. Each file includes one day of data. Further details on the magnetic field measurements can be found in the following reference: Balogh, A., et al., Astron. Astrophys. Suppl. Ser., 92(2), 221, 1992.

This data set contains high resolution samples at about one-hour intervals 1hrof the interplanetary magnetic field measured by the Ulysses Magnetic Field experiment. Field vector components are given in units ofnanoteslas and in RTN coordinates, where R is the radial component or the sun-s/c axis, T is the transverse (along-track) component or the cross product of the solar rotation axis and R, and N is the normal (cross-track) component or the cross product of R and T. The field magnitudes in nT are averages of scalar magnitudes at higher time resolution. Times are computed at the mid-point of each
minute interval and expressed in Spacecraft Event Time - UT (SCET-UT). Data gaps have not been flagged in any way - if there were no available data in a particular hour then there is no data record for that hour. No data from the Feb. 1992 encounter with Jupiter are included. Each file includes one day of data. Further details on the magnetic field measurements can be found in the following reference: Balogh, A., et al., Astron. Astrophys. Suppl. Ser., 92(2), 221, 1992.

This Ulysses GAS experiment data set consists of pixel map data and image files for sky maps generated from GAS measurements in a mode primarily sensitive to ultraviolet photons. The accumulated counts and Ecliptic (spacecraft-centered) angle coordinates for each sky map pixel are given in the ascii files *.TXT. The positions of the Sun and the planets vary with time and with the position of the spacecraft along its trajectory, while the positions of stars remain fixed. The full images are provided in GIF (*.GIF files) and postscript (*.PS files) format, the GIF files being easily viewed on-line (see below) with an Internet web browser. The actual positions of Sun, Earth, and Jupiter are indicated by yellow, green, and white dots, respectively. The area around the Sun is excluded from observation to avoid damaging intensities from direct sunlight.
The files USER_GUIDE.TXT, FORMAT.TXT, and REFERENCE.TXT, respectively, give an overall description of the various datatypes, the record format for the DATA datatype, and a list of GAS-related publications. The users guide defines the nomenclature of the file names.

This Ulysses GAS experiment data set consists of pixel map data and image files for sky maps generated from GAS measurements in the mode primarily sensitive to neutral helium atoms from inflow of interstellar gas into the heliosphere. The accumulated counts and Ecliptic (spacecraft-centered) angle coordinates for each sky map pixel are given in the ascii files *.TXT. The positions of the Sun and the planets vary with time and with the position of the spacecraft along its trajectory, while the positions of stars remain fixed. The full images are provided in GIF (*.GIF files) and postscript (*.PS files) format, the GIF files being easily viewed on-line (see below) with an Internet web browser. The actual positions of Sun, Earth, and Jupiter are indicated by yellow, green and white dots, respectively. The area around the Sun is excluded from observation to avoid damaging intensities from direct sunlight. The files USER_GUIDE.TXT, FORMAT.TXT, and REFERENCE.TXT, respectively, give an overall description of the various datatypes, the record format for the DATA datatype, and a list of GAS-related publications. The users guide defines the nomenclature of the file names. Further details about the data and the experiment may be found in Witte et al., Astron. Astrophys. Suppl. Ser., 92, No. 2, 333-348, 1992 (NSSDC TRF # B40459-000A). Data analysis methods for interstellar helium are described in Banaszkiewicz et al., Astron. Astrophys. Suppl. Ser., 120, 587-602, 1996 (B45706-000A).

Ion and electron fluxes, various time resolutions,
spin-sectored and spin-averaged, ASCII files accessible directly from Fundamental
Technologies or through the Virtual Energetic Particle Observatory (VEPO).

17-min-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEMS30 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Daily-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEMS30 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Hourly-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEMS30 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

17-min-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEFS60 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Daily-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEFS60 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Hourly-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEFS60 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

17-min-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEMS120 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Daily-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEMS120 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Hourly-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the Ulysses/HISCALE LEMS120 instrument.
All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the
solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.